Astronomy:Zeta Tucanae

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Short description: Star in the constellation Tucana
Zeta Tucanae
Location of ζ Tucanae (near center).
Observation data
Equinox J2000.0]] (ICRS)
Constellation Tucana
Right ascension  00h 20m 04.2586s[1]
Declination −64° 52′ 29.257″[1]
Apparent magnitude (V) 4.23[2]
Characteristics
Evolutionary stage main sequence[1]
Spectral type F9.5 V[3]
U−B color index 0.02[4]
B−V color index 0.58[4]
Variable type None[5]
Astrometry
Radial velocity (Rv)9.280±0.0003[6] km/s
Proper motion (μ) RA: 1706.747±0.162[1] mas/yr
Dec.: 1164.959±0.156[1] mas/yr
Parallax (π)116.1826 ± 0.1334[1] mas
Distance28.07 ± 0.03 ly
(8.607 ± 0.010 pc)
Absolute magnitude (MV)4.67[7]
Details
Mass0.985±0.033[8] M☉
Radius1.044±0.010[8] R☉
Luminosity1.232±0.039[8] L☉
Surface gravity (log g)4.394±0.007[8] cgs
Temperature5,924±130[8] K
Metallicity [Fe/H]−0.21±0.09[8] dex
Rotation15.6534±0.0066[9] days
Rotational velocity (v sin i)3.295±0.259[10] km/s
Age5.3±0.5[8] Gyr
Other designations
ζ Tuc, FK5 10, GC 401, GJ 17, HD 1581, HIP 1599, HR 77, SAO 248163, LHS 5, LTT 167[11]
Database references
SIMBADdata

Zeta Tucanae, Latinized from ζ Tucanae, is a star in the constellation Tucana. It is a spectral class F9.5 main sequence star. Based upon parallax measurements by the Hipparcos spacecraft, it is approximately 28.0 light years from Earth.[12] This is one of the least variable stars observed during the Hipparcos mission.[5][13] The star is faintly visible to the naked eye, at an apparent magnitude of +4.23.

Characteristics

Zeta Tucanae is a solar-type star, with similar mass, radius, luminosity, and effective temperature as the Sun, and has an estimated age of 5.3 billion years. Despite having a slightly lower mass, this star is more luminous than the Sun.[8] It is slightly metal-poor,[8] which means the portion of elements heavier than helium is smaller relative to the Sun. The solar-like qualities make it a target of interest for investigating the possible existence of a life-bearing planet.[13]

Zeta Tucanae has a rotation period of 15.65 days,[14][9] and possesses a magnetic activity cycle with period of approximately 950 days.[9][15]

The components of this star's space velocity are U = −60, V = −4 and W = −38 km/s. These correspond to the velocity toward the Galactic Center, the velocity along the direction of galactic rotation, and the velocity toward the north galactic pole, respectively.[16] It is orbiting through the galaxy at a mean distance of 8.4 kpc from the Galactic Center and with an orbital eccentricity of 0.16.[13]

Based upon an excess emission of infrared radiation at 70 micrometres, this system is believed to have a debris disk. It is radiating with a maximum temperature of 218 K, corresponding to a minimum distance from the star of 2.3 astronomical units.[17]

As of 2025, no planet has been discovered in orbit around this star.[9]

See also

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues 2237. Bibcode: 2002yCat.2237....0D. 
  3. ↑ Gray, R. O. et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal 132 (1): 161–170. doi:10.1086/504637. Bibcode: 2006AJ....132..161G. 
  4. ↑ 4.0 4.1 Johnson, H. L.; Iriarte, B.; Mitchell, R. I.; Wisniewskj, W. Z. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory 4 (99): 99. Bibcode: 1966CoLPL...4...99J. 
  5. ↑ 5.0 5.1 Adelman, S. J. (February 2001). "Research Note Hipparcos photometry: The least variable stars". Astronomy and Astrophysics 367 (1): 297–298. doi:10.1051/0004-6361:20000567. Bibcode: 2001A&A...367..297A. 
  6. ↑ Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  7. ↑ Elgarøy, Øystein; Engvold, Oddbjørn; Lund, Niels (March 1999). "The Wilson-Bappu effect of the MgII K line - dependence on stellar temperature, activity and metallicity". Astronomy and Astrophysics 343: 222–228. Bibcode: 1999A&A...343..222E. 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 8.5 8.6 8.7 8.8 Huber, Daniel et al. (2022-02-01). "A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c". The Astronomical Journal 163 (2): 79. doi:10.3847/1538-3881/ac3000. ISSN 0004-6256. Bibcode: 2022AJ....163...79H. 
  9. ↑ 9.0 9.1 9.2 9.3 Harada, Caleb K.; Dressing, Courtney D.; Kane, Stephen R.; Blunt, Sarah; Dietrich, Jamie; Hinkel, Natalie R.; Li, Zhexing; Mamajek, Eric; Rice, Malena; Tuchow, Noah W.; Turtelboom, Emma V.; Wittenmyer, Robert A. (2024-09-16). "SPORES-HWO. II. Limits on Planetary Companions of Future High-contrast Imaging Targets from $>$20 Years of HIRES and HARPS Radial Velocities". arXiv:2409.10679 [astro-ph.EP].
  10. ↑ Perdelwitz, V.; Trifonov, T.; Teklu, J. T.; Sreenivas, K. R.; Tal-Or, L. (2024). "Analysis of the public HARPS/ESO spectroscopic archive". Astronomy & Astrophysics (EDP Sciences) 683: A125. doi:10.1051/0004-6361/202348263. ISSN 0004-6361. Bibcode: 2024A&A...683A.125P. https://www.aanda.org/articles/aa/pdf/2024/03/aa48263-23.pdf. Retrieved 2025-08-13. 
  11. ↑ "zet Tuc -- High Proper Motion Star". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Zeta+Tucanae. 
  12. ↑ van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V  Note: see VizieR catalogue I/311.
  13. ↑ 13.0 13.1 13.2 Porto de Mello, Gustavo; del Peloso, Eduardo F.; Ghezzi, Luan (2006). "Astrobiologically Interesting Stars Within 10 Parsecs of the Sun". Astrobiology 6 (2): 308–331. doi:10.1089/ast.2006.6.308. PMID 16689649. Bibcode: 2006AsBio...6..308P. 
  14. ↑ Laliotis, Katherine; Burt, Jennifer A.; Mamajek, Eric E.; Li, Zhexing; Perdelwitz, Volker; Zhao, Jinglin; Butler, R. Paul; Holden, Bradford et al. (2023-04-01). "Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions". The Astronomical Journal 165 (4): 176. doi:10.3847/1538-3881/acc067. ISSN 0004-6256. Bibcode: 2023AJ....165..176L. 
  15. ↑ Lovis, C.; Dumusque, X.; Santos, N. C.; Bouchy, F.; Mayor, M.; Pepe, F.; Queloz, D.; Ségransan, D.; Udry, S. (2011-07-26). "The HARPS search for southern extra-solar planets. XXXI. Magnetic activity cycles in solar-type stars: statistics and impact on precise radial velocities". arXiv:1107.5325 [astro-ph.SR].
  16. ↑ Woolley, Richard van der Riet (1970). "Catalogue of Stars within 25 Parsecs of the Sun". Royal Observatory Annals (Herstmonceux, Royal Greenwich Observatory) 5. http://heasarc.gsfc.nasa.gov/W3Browse/all/woolley.html. Retrieved 2009-09-02. 
  17. ↑ Trilling, D. E. (2008). "Debris Disks around Sun-like Stars". The Astrophysical Journal 674 (2): 1086–1105. doi:10.1086/525514. Bibcode: 2008ApJ...674.1086T. 



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